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dc.contributor.authorHall, Cassandra
dc.contributor.authorForgan, Duncan
dc.contributor.authorRice, Ken
dc.date.accessioned2017-07-26T11:30:12Z
dc.date.available2017-07-26T11:30:12Z
dc.date.issued2017-09-21
dc.identifier.citationHall , C , Forgan , D & Rice , K 2017 , ' Identifying and analysing protostellar disc fragments in smoothed particle hydrodynamics simulations ' Monthly Notices of the Royal Astronomical Society , vol. 470 , no. 3 , pp. 2517-2538 . https://doi.org/10.1093/mnras/stx1244en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 250565544
dc.identifier.otherPURE UUID: ce281afc-db22-4c7a-b475-4cc762d49f57
dc.identifier.otherScopus: 85023759034
dc.identifier.otherWOS: 000406844800001
dc.identifier.urihttp://hdl.handle.net/10023/11288
dc.descriptionKR gratefully acknowledges support from STFC grant ST/M001229/1. DF gratefully acknowledges support from the ECOGAL project, grant agreement 291227, funded by the European Research Council under ERC-2011-ADG. The research leading to these results also received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 681601).en
dc.description.abstractWe present a new method of identifying protostellar disc fragments in a simulation based on density derivatives, and analyse our data using this and the existing CLUMPFIND method,which is based on an ordered search over all particles in gravitational potential energy. Using smoothed particle hydrodynamics, we carry out nine simulations of a 0.25 M⊙ disc around a1 M⊙ star, all of which fragment to form at least two bound objects. We find that when using all particles ordered in gravitational potential space, only fragments that survive the duration of the simulation are detected. When we use the density derivative method, all fragments are detected, so the two methods are complementary, as using the two methods together allows us to identify all fragments, and to then determine those that are likely to be destroyed. We find a tentative empirical relationship between the dominant azimuthal wavenumber in the disc m and the maximum semimajor axis a fragment may achieve in a simulation, such that amax α 1/m. We find the fragment destruction rate to be around half that predicted from population synthesis models. This is due to fragment-fragment interactions in the early gas phase of the disc, which can cause scattering and eccentricity pumping on short time-scales, and affects the fragment's internal structure. We therefore caution that measurements of eccentricity as a function of semimajor axis may not necessarily constrain the formation mechanism of giant planets and brown dwarfs.
dc.format.extent22
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1093/mnras/stx1244en
dc.subjectBrown dwarfsen
dc.subjectDisc interactionsen
dc.subjectHydrodynamicsen
dc.subjectPlaneten
dc.subjectPlanetary systemsen
dc.subjectPlanets and satellites: dynamical evolution and stabilityen
dc.subjectProtoplanetary discsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleIdentifying and analysing protostellar disc fragments in smoothed particle hydrodynamics simulationsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stx1244
dc.description.statusPeer revieweden


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